The presence of copious amounts of dust in high redshift galaxies may be explained by core collapse supernovae (CCSNe). The dust in high-z galaxies must come from young, massive stars, so CCSNe are one of the few possible sources. We propose to begin monitoring three bright new CCSNe (SNe 2010F, 2010K, and 2010as) to look for signatures of dust formation, as well as continue the monitoring of the three dust-producing SNe 2004et, 2007it, and 2007od. The three observational signatures of this dust formation include, a decrease in the continuum brightness in the visible, a developing infrared excess, and asymmetric, blue-shifted emission-line profiles. With Spitzer, we will be able to carefully study the IR emission, and put strong constraints on the dust mass and how the dust changes with time. The proposed observations will be combined with previous epochs of Spitzer data and coordinated with other approved and proposed ground and space based observations with Magellan, Gemini, and HST. We may be able to increase the small sample of CCSNe that show all three signatures of dust formation, as well as constrain pre-existing progenitor dust creation by studying the IR echoes around the older SNe. These observations will help us to better understand what fraction of CCSNe produce dust, how much dust they produce, and how CCSNe behave at late times. These estimates will help us to deduce whether CCSNe can be a major source of dust in young, high redshift galaxies.
- Pub Date:
- June 2010